  The formation of circumstellar disks is investigated using three-dimensional
resistive magnetohydrodynamic simulations, in which the initial prestellar
cloud has a misaligned rotation axis with respect to the magnetic field. We
examine the effects of (i) the initial angle difference between the global
magnetic field and the cloud rotation axis ($\theta_0$) and (ii) the ratio of
the thermal to gravitational energy ($\alpha_0$). We study $16$ models in total
and calculate the cloud evolution until $\sim \! 5000$ yr after protostar
formation. Our simulation results indicate that an initial non-zero $\theta_0$
($> 0$) promotes the disk formation but tends to suppress the outflow driving,
for models that are moderately gravitationally unstable, $\alpha_0 \lesssim 1$.
In these models, a large-sized rotationally-supported disk forms and a weak
outflow appears, in contrast to a smaller disk and strong outflow in the
aligned case ($\theta_0 = 0$). Furthermore, we find that when the initial cloud
is highly unstable with small $\alpha_0$, the initial angle difference
$\theta_0$ does not significantly affect the disk formation and outflow
driving.
