  We present average stellar population properties and dark matter halo masses
of $z \sim 2$ \lya emitters (LAEs) from SED fitting and clustering analysis,
respectively, using $\simeq$ $1250$ objects ($NB387\le25.5$) in four separate
fields of $\simeq 1$ deg$^2$ in total. With an average stellar mass of $10.2\,
\pm\, 1.8\times 10^8\ {\mathrm M_\odot}$ and star formation rate of $3.4\,
\pm\, 0.4\ {\mathrm M_\odot}\ {\rm yr^{-1}}$, the LAEs lie on an extrapolation
of the star-formation main sequence (MS) to low stellar mass. Their effective
dark matter halo mass is estimated to be $4.0_{-2.9}^{+5.1} \times 10^{10}\
{\mathrm M_\odot}$ with an effective bias of $1.22^{+0.16}_{-0.18}$ which is
lower than that of $z \sim 2$ LAEs ($1.8\, \pm\, 0.3$), obtained by a previous
study based on a three times smaller survey area, with a probability of $96\%$.
However, the difference in the bias values can be explained if cosmic variance
is taken into account. If such a low halo mass implies a low HI gas mass, this
result appears to be consistent with the observations of a high \lya escape
fraction. With the low halo masses and ongoing star formation, our LAEs have a
relatively high stellar-to-halo mass ratio (SHMR) and a high efficiency of
converting baryons into stars. The extended Press-Schechter formalism predicts
that at $z=0$ our LAEs are typically embedded in halos with masses similar to
that of the Large Magellanic Cloud (LMC); they will also have similar SHMRs to
the LMC, if their SFRs are largely suppressed after $z \sim 2$ as some previous
studies have reported for the LMC itself.
