  In this work, we provide 2189 photometric- and kinematic-selected member
candidates of 24 star clusters from the LAMOST DR2 catalog. We perform two-step
membership identification: selection along the stellar track in the
color-magnitude diagram, i.e., photometric identification, and the selection
from the distribution of radial velocities, i.e. the kinematic identification.
We find that the radial velocity from the LAMOST data are very helpful in the
membership identification. The mean probability of membership is 40\% for the
radial velocity selected sample. With these 24 star clusters, we investigate
the performance of the radial velocity and metallicity estimated in the LAMOST
pipeline. We find that the systematic offset in radial velocity and metallicity
are $0.85\pm1.26$\,\kms\ and $-0.08\pm0.04$\,dex, with dispersions of
$5.47_{-0.71}^{+1.16}$\,\kms\ and $0.13_{-0.02}^{+0.04}$\,dex, respectively.
Finally, we propose that the photometric member candidates of the clusters
covered by the LAMOST footprints should be assigned higher priority so that
more member stars can be observed.
