  Recent observations suggest that intensive molecular cloud collision can
trigger massive star/cluster formation. The most important physical process
caused by the collision is a shock compression. In this paper, the influence of
a shock wave on the evolution of a molecular cloud is studied numerically by
using isothermal magnetohydrodynamics (MHD) simulations with the effect of
self-gravity. Adaptive-mesh-refinement and sink particle techniques are used to
follow long-time evolution of the shocked cloud. We find that the shock
compression of turbulent inhomogeneous molecular cloud creates massive
filaments, which lie perpendicularly to the background magnetic field as we
have pointed out in a previous paper. The massive filament shows global
collapse along the filament, which feeds a sink particle located at the
collapse center. We observe high accretion rate dot{M}_acc > 10^{-4} M_sun/yr
that is high enough to allow the formation of even O-type stars. The most
massive sink particle achieves M>50 M_sun in a few times 10^5 yr after the
onset of the filament collapse.
