  We present the clustering analysis of photometric luminous red galaxies
(LRGs) at a broad redshift range, $0.1 \leq z \leq 1.05$, selected in the Hyper
Suprime-Cam Subaru Strategic Program Wide layer. The CAMIRA algorithm yields
$615,317$ LRGs over $\sim 124$ deg$^{2}$ with information of stellar masses and
photometric redshifts, enabling to trace the redshift and stellar-mass
dependence of the baryonic and dark halo characteristics of LRGs. The halo
occupation distribution analysis reveals a tight correlation between the dark
halo mass of central LRGs, $M_{\rm min}$, and the number density of LRGs
independently of redshifts, indicating that the formation of LRGs is associated
with the global environment. The halo mass $M_{\rm min}$ of the LRGs depends
only weakly on the stellar mass $M_{\star}$ at $M_{\star} \lesssim
10^{10.75}h^{-2}M_{\odot}$ and $0.3<z<1.05$, in contrast to the $M_{\rm
min}$--$M_{\star}$ relation for all galaxies including both red and blue
galaxies. This is indicative of the dark halo mass is being the key parameter
for the formation of LRGs rather than the stellar mass. Our result suggests
that the halo mass of $\sim 10^{12.5\pm0.2}h^{-1}M_{\odot}$ is the critical
mass for an efficient halo quenching due to the halo environment. A comparison
between our observed halo masses and the hydrodynamical simulation indicates
that the low-mass LRGs at $z\sim1$ increase their stellar masses one order
magnitude across $z=1-0$ through mergers and satellite accretions, and large
fraction of massive LRGs at $z<0.9$ evolve from massive green valley galaxies
with short transition time scale.
