  We study the angular correlation function of star-forming galaxies and
properties of their host dark matter halos at $z>1$ using the Subaru
Hyper-Suprime Cam (HSC) survey. We use [OII] emitters identified using two
narrow-band (NB) filters, NB816 and NB921, in the Deep/UltraDeep layers, which
respectively cover large angular areas of $16.3 ~{\rm deg}^2$ and $16.9~{\rm
deg}^2$. Our sample contains 8302 and 9578 [OII] emitters at $z=1.19$ (NB816)
and $z=1.47$ (NB921), respectively. We detect a strong clustering signal over a
wide angular range, $0.001 < \theta < 1$ [deg], with the bias
$b=1.61^{+0.13}_{-0.11}$ ($z=1.19$) and $b=2.09^{+0.17}_{-0.15}$ ($z=1.47$). We
also find the clear deviation of the correlation from a simple power-law form.
To interpret the measured clustering signal, we adopt a halo occupation
distribution (HOD) model which is constructed to explain the spatial
distribution of galaxies selected by a star formation rate. The observed
correlation function and number density are simultaneously explained by the
best-fitting HOD model. From the constrained HOD model, the average mass of
halos hosting the [OII] emitters is derived to be $\log{M_{\rm
  eff}/(h^{-1}M_\odot)}=12.70^{+0.09}_{-0.07}$ and $12.61^{+0.09}_{-0.05}$ at
$z=1.19$ and $1.47$, respectively, which will become halos with the present-day
mass, $M\sim 1.5 \times 10^{13}h^{-1}M_\odot$. The satellite fraction of the
[OII] emitter sample is found to be $f_{\rm sat}\sim 0.15$. All these values
are consistent with the previous studies of similar samples, but we obtain
tighter constraints due to the high number density and large angular coverage
of our sample. The results obtained for host halos of [OII] emitters in this
paper are expected to be applicable to upcoming emission line galaxy surveys
such as the Subaru Prime Focus Spectrograph survey.
