  Stars form in dense cores of molecular clouds that are observed to be
significantly magnetized. In the simplest case of a laminar (non-turbulent)
core with the magnetic field aligned with the rotation axis, both analytic
considerations and numerical simulations have shown that the formation of a
large, $10^2\au$-scale, rotationally supported protostellar disk is suppressed
by magnetic braking in the ideal MHD limit for a realistic level of core
magnetization. This theoretical difficulty in forming protostellar disks is
termed "magnetic braking catastrophe". A possible resolution to this problem,
proposed by \citeauthor{HennebelleCiardi2009} and \citeauthor{Joos+2012}, is
that misalignment between the magnetic field and rotation axis may weaken the
magnetic braking enough to enable disk formation. We evaluate this possibility
quantitatively through numerical simulations. We confirm the basic result of
\citeauthor{Joos+2012} that the misalignment is indeed conducive to disk
formation. In relatively weakly magnetized cores with dimensionless
mass-to-flux ratio $\gtrsim 5$, it enabled the formation of rotationally
supported disks that would otherwise be suppressed if the magnetic field and
rotation axis are aligned. For more strongly magnetized cores, disk formation
remains suppressed, however, even for the maximum tilt angle of $90\degree$. If
dense cores are as strongly magnetized as indicated by OH Zeeman observations
(with a mean dimensionless mass-to-flux ratio $\sim 2$), it would be difficult
for the misalignment alone to enable disk formation in the majority of them. We
conclude that, while beneficial to disk formation, especially for the
relatively weak field case, the misalignment does not completely solve the
problem of catastrophic magnetic braking in general.
