  In this work, we use measurements of galaxy stellar mass and two-point
angular correlation functions to constrain the stellar-to-halo mass ratios
(SHMRs) of passive and \np\ galaxies at $z\sim2-3$, as identified in the
\emph{Spitzer} Matching Survey of the UltraVISTA ultra-deep Stripes (SMUVS). We
adopt a sophisticated halo modeling approach to statistically divide our two
populations into central and satellite galaxies. For central galaxies, we find
that the normalization of the SHMR is greater for our passive population.
Through the modeling of $\Lambda$ cold dark matter halo mass accretion
histories, we show that this can only arise if the conversion of baryons into
stars was more efficient at higher redshifts and additionally that passive
galaxies can be plausibly explained as residing in halos with the highest
formation redshifts (i.e., those with the lowest accretion rates) at a given
halo mass. At a fixed stellar mass, satellite galaxies occupy host halos with a
greater mass than central galaxies, and we find further that the fraction of
passive galaxies that are satellites is higher than for the combined
population. This, and our derived satellite quenching timescales, combined with
earlier estimates from the literature, support dynamical/environmental
mechanisms as the dominant process for satellite quenching at $z\lesssim3$.
