The formation of the magnetotail configuration under the influence of the solar wind plasma flow entering the magnetosphere and the associated driven reconnection in the magnetotail region are studied numerically by means of a two-dimensional time-dependent nonlinear resistive MHD code. The initial magnetic field is generated by a two-dimensional dipole, and the initial plasma pressure is assumed uniform. As the solar wind plasmas move in the tailward direction, the magnetic field lines are stretched so that a two-dimensional tail-like configuration is formed. Plasma sheet thinning is observed during the further development of tail formation. When the magnetic field line is stretched and hence the neutral sheet current is enhanced enough, x-type reconnection is triggered in the presence of resistivity. Plasmoid is formed in the downstream region and is accelerated along the sun-earth line as a consequence of reconnection. A moderate earthward and strong tailward plasma jetting is also observed. Dependence of the simulation results on the resistivity and the solar wind energy flux is discussed in detail. The reconnection rate does not depend on resistivity, but the resistivity influences the onset time of reconnection. In contrast, the reconnection rate is very sensitive to the incoming solar wind speed. A broad current sheet is formed in the neutral region in the present case rather than a pair of sharply peaked current sheets, which were observed in the previous simulation studies in which the initial configuration was one-dimensional.