We perform SubHalo Abundance Matching (SHAM) studies on UNIT simulations with {sigma, V-ceil, v(smear)}-SHAM and {sigma, V-ceil, f(sat)}-SHAM. They are designed to reproduce the clustering on 5-30 h(-1) Mpc of luminous red galaxies (LRGs), emission-line galaxies (ELGs), and quasi-stellar objects (QSOs) at 0.4 < z < 3.5 from DESI (Dark Energy Spectroscopic Instrument) One Percent Survey. V-ceil is the incompleteness of the massive host (sub)haloes and is the key to the generalized SHAM. v(smear) models the clustering effect of redshift uncertainties, providing measurements consistent with those from repeat observations. A free satellite fraction f(sat) is necessary to reproduce the clustering of ELGs. We find ELGs present a more complex galaxy-halo mass relation than LRGs reflected in their weak constraints on sigma. LRGs, QSOs, and ELGs show increasing V-ceil values, corresponding to the massive galaxy incompleteness of LRGs, the quenched star formation of ELGs and the quenched black hole accretion of QSOs. For LRGs, a Gaussian v(smear) presents a better profile for subsamples at redshift bins than a Lorentzian profile used for other tracers. The impact of the statistical redshift uncertainty on ELG clustering is negligible. The best-fitting satellite fraction for DESI ELGs is around 4 per cent, lower than previous estimations for ELGs. The mean halo mass log(10)(< M-vir >) in h(-1) M-circle dot for LRGs, ELGs, and QSOs are 13.16 +/- 0.01, 11.90 +/- 0.06, and 12.66 +/- 0.45, respectively. Our generalized SHAM algorithms facilitate the production of multitracer galaxy mocks for cosmological tests.