  The \emph{Spitzer} Matching Survey of the UltraVISTA ultra-deep Stripes
(SMUVS) provides unparalleled depth at $3.6$ and $4.5$~$\mu$m over
$\sim0.66$~deg$^2$ of the COSMOS field, allowing precise photometric
determinations of redshift and stellar mass. From this unique dataset we can
connect galaxy samples, selected by stellar mass, to their host dark matter
halos for $1.5<z<5.0$, filling in a large hitherto unexplored region of the
parameter space. To interpret the observed galaxy clustering we utilize a
phenomenological halo model, combined with a novel method to account for
uncertainties arising from the use of photometric redshifts. We find that the
satellite fraction decreases with increasing redshift and that the clustering
amplitude (e.g., comoving correlation length / large-scale bias) displays
monotonic trends with redshift and stellar mass. Applying $\Lambda$CDM halo
mass accretion histories and cumulative abundance arguments for the evolution
of stellar mass content we propose pathways for the coevolution of dark matter
and stellar mass assembly. Additionally, we are able to estimate that the halo
mass at which the ratio of stellar to halo mass is maximized is
$10^{12.5_{-0.08}^{+0.10}}$~M$_{\odot}$ at $z\sim2.5$. This peak halo mass is
here inferred for the first time from stellar mass-selected clustering
measurements at $z\gtrsim2$, and implies mild evolution of this quantity for
$z\lesssim3$, consistent with constraints from abundance-matching techniques.
