  We investigate the possibility of the growth of magnetorotational instability
(MRI) in disks around Class 0 protostars. We construct a disk model and
calculate the chemical reactions of neutral and charged atoms, molecules and
dust grains to derive the abundance of each species and the ionization degree
of the disk. Then, we estimate the diffusion coefficients of non-ideal
magnetohydrodynamics effects such as ohmic dissipation, ambipolar diffusion and
the Hall effect. Finally, we evaluate the linear growth rate of MRI in each
area of the disk. We investigate the effect of changes in the strength and
direction of the magnetic field in our disk model and we adopt four different
dust models to investigate the effect of dust size distribution on the
diffusion coefficients. Our results indicate that an MRI active region possibly
exists with a weak magnetic field in a region far from the protostar where the
Hall effect plays a role in the growth of MRI. On the other hand, in all models
the disk is stable against MRI in the region within $<20$ au from the protostar
on the equatorial plane. Since the size of the disks in the early stage of star
formation is limited to $\lesssim 10-$$20$ au, it is difficult to develop
MRI-driven turbulence in such disks.
