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 _ { 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 % .

( 3 ) Repetitive interaction between the Clouds and the Galaxy enhances moderately the star formation rate to \sim 0.4 M _ { \odot } yr ^ { -1 } in the LMC disk .
Most of the new stars ( \sim 90 % ) are formed within the central 3 kpc of the disk , in particular , within the central bar for the last 9 Gyr .
Consequently , the half mass radius is different by a factor of 2.3 between old field stars and newly formed ones .

( 4 ) Efficient globular cluster formation does not occur until the LMC starts interacting violently and closely with the SMC ( \sim 3 Gyrs ago ) .
The newly formed globular cluster system has a disky distribution with rotational kinematics and its mean metallicity is \sim 1.2 higher than that of new field stars because of the pre-enrichment by the formation of field stars prior to cluster formation .

( 5 ) The LMC evolution depends on its initial mass and orbit with respect to the Galaxy and the SMC .
In particular , the epoch of the bar and thick disk formation and the mass fraction of the stellar halo depend on the initial mass of the LMC .

Based on these results , we discuss the entire formation history of the LMC , the possible fossil records of past interaction between the Clouds and the Galaxy , and the star formation history of the SMC for the last several Gyr .