  We present the clustering analysis of photometric luminous red galaxies
(LRGs) at a redshift range of $0.1\leq z \leq 1.05$ using $615,317$ photometric
LRGs selected from the Hyper Suprime-Cam Subaru Strategic Program covering
$\sim124$ deg$^{2}$. Our sample covers a broad range of stellar masses and
photometric redshifts and enables a halo occupation distribution analysis to
study the redshift and stellar-mass dependence of dark halo properties of LRGs.
We find a tight correlation between the characteristic dark halo mass to host
central LRGs, $M_{\min}$, and the number density of LRGs independently of
redshifts, indicating that the formation of LRGs is associated with the global
environment. The $M_{\min}$ of LRGs depends only weakly on the stellar mass
$M_{\star}$ at $M_{\star} \lesssim 10^{10.75}h^{-2} M_{\odot}$ at $0.3<z<1.05$,
in contrast to the case for all photometrically selected galaxies for which
$M_{\min}$ shows significant dependence on $M_{\star}$ even at low $M_{\star}$.
The weak stellar mass dependence is indicative of the dark halo mass being the
key parameter for the formation of LRGs rather than the stellar mass. Our
result suggests that the halo mass of $\sim 10^{12.5 \pm 0.2}h^{-1} M_{\odot}$
is the critical mass for an efficient halo quenching due to the halo
environment. We compare our result with the result of the hydrodynamical
simulation to find that low-mass LRGs at $z \sim 1$ will increase their stellar
masses by an order magnitude from $z=1$ to $0$ through mergers and satellite
accretions, and a large fraction of massive LRGs at $z<0.9$ consist of LRGs
that are recently migrated from massive green valley galaxies or those evolved
from less massive LRGs through mergers and satellite accretions.
