  We infer the connection between the stellar mass of galaxies from the Subaru
Hyper Suprime-Cam (HSC) survey, and their dark matter halo masses and its
evolution in two bins of redshifts between $[0.3, 0.8]$. We use the
measurements of the weak lensing signal of galaxies using background sources
from the Year 1 shape catalog from the HSC survey. We bin galaxies in stellar
mass with varying thresholds ranging from $8.6 \leq \log [ M_*/(h^{-2}
{M_\odot})] \leq 11.2$ and use stringent cuts in the selection of source
galaxies to measure the weak lensing signal. We model these measurements of the
weak lensing signal together with the abundance of galaxies in the halo
occupation distribution framework. We obtain constraints on the halo occupation
parameters of central galaxies $M_{\rm min}$ and $\sigma_{\log M}$, which
correspond to the halo mass at which central galaxies for each threshold sample
reach half occupancy, and its scatter, respectively, along with parameters that
describe the occupation of the satellite galaxies. The measurements of
abundance and weak lensing individually constrain different degeneracy
directions in the $M_{\rm min}$ and $\sigma_{\log M}$ plane, thus breaking the
degeneracy in these parameters. We demonstrate that the weak lensing
measurements are best able to constrain the average central halo masses,
$\langle M_{\rm cen} \rangle$. We compare our measurements to those obtained
using the abundance and clustering of these galaxies as well as the subhalo
abundance matching measurements and demonstrate qualitative agreement. We find
that the galaxy-dark matter connection does not vary significantly between
redshift bins we explore in this study. Uncertainties in the photometric
redshift of the lens galaxies imply that more efforts are required to
understand the true underlying stellar mass-halo mass relation of galaxies and
its evolution over cosmic epoch.
