In order to clarify the physics behind the diverse observed cases, it is necessary to construct a theoretical model of the star formation process and compare it with observations at different scales and evolutionary stages. However, the numerical simulations have not reached the same stage as the currently observed Class 0/I protostar-forming regions, so it has been challenging to directly compare the physical properties obtained by observations and simulations. We calculate the star formation process up to 100,000 years after protostar formation using a non-ideal magnetohydrodynamic code. We study whether we can reproduce the observed diversity of star formation regions by varying (1) the magnetic field strength and (2) the direction of the magnetic field lines relative to the molecular cloud rotation axis as parameters to the uniform magnetic field given to the molecular cloud, which is the initial condition of the calculation. This poster focuses on the issue of dynamical structure, in which the infall velocity of the accreting envelope is 0.3-0.5 times smaller than the free-fall velocity. This difference calls into question the dynamical model of the envelope assumed when estimating protostellar masses, but the origin was unclear. From the present calculation, we confirm that the infall velocity decreases in the false disk region (~ 1000 [au]), which exists outside the Keplerian disk, and that it is smaller depending on (1) the magnetic field strength, (2) the direction of the magnetic field, and (3) the evolutionary stage. Three factors explain the cause of the decrease in the fall velocity and the dispersion of the decrease rate among the observed sources.