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We present the clustering properties of low-$z$ $(z\leq1.4)$ galaxiesselected by the Hyper Suprime-Cam Subaru Strategic Program Wide layer over$145$ deg$^{2}$. The wide-field and multi-wavelength observation yields$5,064,770$ galaxies at $0.3\leq z\leq1.4$ with photometric redshifts andphysical properties. This enables the accurate measurement of angularcorrelation functions and subsequent halo occupation distribution (HOD)analysis allows the connection between baryonic properties and dark haloproperties. The fraction of less-massive satellite galaxies at $z\lesssim1$ isfound to be almost constant at $\sim20\%$, but it gradually decreases beyond$M_{\star} \sim 10^{10.4}h^{-2}M_{\odot}$. However, the abundance of satellitegalaxies at $z>1$ is quite small even for less-massive galaxies due to therarity of massive centrals at high-$z$. This decreasing trend is connected tothe small satellite fraction of Lyman break galaxies at $z>3$. Thestellar-to-halo mass ratios at $0.3\leq z\leq1.4$ are almost consistent withthe predictions obtained using the latest empirical model; however, we identifysmall excesses from the theoretical model at the massive end. The pivot halomass is found to be unchanged at $10^{11.9-12.1}h^{-1}M_{\odot}$ at $0.3\leqz\leq1.4$, and we systematically show that $10^{12}h^{-1}M_{\odot}$ is auniversal pivot halo mass up to $z\sim5$ that is derived using only theclustering/HOD analyses. Nevertheless, halo masses with peaked instantaneousbaryon conversion efficiencies are much smaller than the pivot halo massregardless of a redshift, and the most efficient stellar-mass assembly isthought to be in progress in $10^{11.0-11.5}h^{-1}M_{\odot}$ dark haloes.

The Subaru HSC Galaxy Clustering with Photometric Redshift I: Dark Halo Masses Versus Baryonic Properties of Galaxies at 0.3