  Dynamical contraction of a slowly-rotating magnetized cloud is studied using
the magnetohydrodynamical (MHD) simulations. In the isothermal stage ($n \la
n_{\rm A} \sim 10^{10}{\rm cm}^{-3}$), the cloud evolves similarly to that
expected from Larson-Penston self-similar solution and experiences the run-away
collapse. However, after the central density exceeds $\sim n_{\rm A}$, an
accretion disk is formed around the adiabatic core. Just outside the core,
outflow is ejected by the effect of magnetic torque (magnetocentrifugal wind).
Since $\sim$ 10% of the mass is ejected with almost all the angular momentum,
the specific angular momentum of the protostellar core reduces to that observed
in main-sequence stars.
