  We investigate the dynamical and chemical evolution of the Large Magellanic
Cloud (LMC) interacting with the Galaxy and the Small Magellanic Cloud (SMC)
based on a series of self-consistent chemodynamical simulations. Our numerical
models are aimed at explaining the entire properties of the LMC, i.e., the
observed structure and kinematics of its stellar halo and disk components as
well as the populations of the field stars and star clusters. The main results
of the present simulations are summarized as follows. (1) Tidal interaction
between the Clouds and the Galaxy during the last 9 Gyr transforms the
initially thin, non-barred LMC disk into the three different components: the
central bar, thick disk, and kinematically hot stellar halo. The central bar is
composed both of old field stars and newly formed ones with each fraction being
equal in its innermost part. The final thick disk has the central velocity
dispersion of $\sim$ 30 km s$^{-1}$ and shows rotationally supported kinematics
with $V_{\rm m}/{\sigma}_{0}$ $\sim$ 2.3. (2) The stellar halo is formed during
the interaction, consisting mainly of old stars originating from the outer part
of the initially thin LMC disk. The outer halo shows velocity dispersion of
$\sim$ 40 km s$^{-1}$ at the distance of 7.5 kpc from the LMC center and has
somewhat inhomogeneous distribution of stars. The stellar halo contains
relatively young, metal-rich stars with the mass fraction of 2 %.
