  We discuss structural and kinematical properties of the stellar halo and the
old globular cluster system (GCS) in the Large Magellanic Cloud (LMC) based on
numerical simulations of the LMC formation. We particularly discuss the
observed possible GCS's rotational kinematics (V/sigma > 2) that appears to be
significantly different from the stellar halo's one with a large velocity
dispersion (~50 km/s). We consider that both halo field stars and old GCs can
originate from low-mass subhalos virialized at high redshifts (z >6). We
investigate the final dynamical properties of the two old components in the
LMC's halo formed from merging of low-mass subhalos with field stars and GCs.
We find that the GCS composed of old globular clusters (GCs) formed at high
redshifts (z > 6) has little rotation (V/sigma ~0.4) and structure and
kinematics similar to those of the stellar halo. This inconsistency between the
simulated GCS's kinematics and the observed one is found to be seen in models
with different parameters. This inconsistency therefore implies that if old,
metal-poor GCs in the LMC have rotational kinematics, they are highly unlikely
to originate from the low-mass subhalos that formed the stellar halo. We thus
discuss a scenario in which the stellar halo was formed from low-mass subhalos
with no/few GCs whereas the GCS was formed at the very early epoch of the LMC's
disk formation via dissipative minor and major merging of gas-rich subhalos and
gas infall. We suggest that there can be a threshold subhalo mass above which
GCs can be formed within subhalos at high redshifts and thus that this
threshold causes differences in physical properties between stellar halos and
GCSs in less luminous galaxies like the LMC.
