Context. Investigating the ionizing emission of star-forming galaxies and the escape fraction of ionizing photons is critical to understanding their contribution to reionization and their impact on the surrounding environment. The number of ionizing photons available to reionize the intergalactic medium (IGM) depends on not only the abundance of galaxies but also their efficiency in producing ionizing photons (xi(ion)). This quantity is thus fundamental to quantify the role of faint versus bright sources in driving this process, as we must assess their relative contribution to the total ionizing emissivity. Aims. Our goal is to estimate the xi(ion) using Balmer lines (H alpha or H beta) in a sample of 761 galaxies at 4 <= z <= 10 selected from different JWST spectroscopic surveys. We aim to determine the redshift evolution of xi(ion) and the relation of xi(ion) with the physical properties of the galaxies. Methods. We used the available HST and JWST photometry to perform a spectral energy distribution (SED) fitting in the sample to determine their physical properties and relate them with xi(ion). We used the BAGPIPES code for the SED fitting and assumed a delayed exponential model for the star formation history. We used the NIRSpec spectra from prism or grating configurations to estimate Balmer luminosities, and then constrained xi(ion) values after dust correction. Results. We find a mean value of 10(25.22) Hz erg(-1) for xi(ion) in the sample with an observed scatter of 0.42 dex. We find an increase in the median values of xi(ion) with redshift from 10(25.09) Hz erg(-1) at z similar to 4.18 to 10(25.28) Hz erg(-1) at z similar to 7.14, confirming the redshift evolution of xi(ion) found in other studies. Regarding the relation between xi(ion) and physical properties, we find a decrease in xi(ion) with increasing stellar mass, indicating that low-mass galaxies are efficient producers of ionizing photons. We also find an increase in xi(ion) with increasing specific star formation rate (sSFR) and increasing UV absolute magnitude. This indicates that faint galaxies and galaxies with high sSFR are also efficient producers. We also investigated the relation of xi(ion) with the rest-frame equivalent width (EW) of [OIII]lambda 5007 and find that galaxies with the higher EW([OIII]lambda 5007) are more efficient producers of ionizing photons, with the best fit leading to the relation log(xi(ion)) = 0.43 x log(EW[OIII])+23.99. Similarly, we find that galaxies with higher O32 = [OIII]lambda 5007/[OII]lambda lambda 3727,3729 and lower gas-phase metallicities (based on the R23 = ([OIII]lambda lambda 4959,5007+[OII]lambda lambda 3727,3729)/H beta calibration) show higher xi(ion) values.