  Gaseous circumbinary disks (CBDs) that are highly inclined to the binary
orbit are commonly observed in nature. These disks harbor particles that can
reach large mutual inclinations as a result of nodal precession once the gas
disk has dissipated. With n-body simulations that include fragmentation we
demonstrate that misaligned disks of particles can be efficient progenitors of
interstellar asteroids (ISAs). Collisions that take place between particles
with large mutual inclinations have large impact velocities which can result in
mass ejection, with a wide range of fragment sizes and ejection velocities. We
explore the binary parameters for which the majority of the terrestrial planet
forming material is ejected rather than accreted into planets. The misalignment
required to eject significant material decreases with binary eccentricity. If
the distribution of binary eccentricity is uniform and the initial particle CBD
orientation relative to the binary orbit is isotropic, about 59% of binaries
are more likely to eject the majority of their CBD terrestrial planet disk mass
through high velocity body-body collisions rather than retain this material and
build terrestrial planets. However, binary--disk interactions during the gas
disk phase with non-zero disk viscosity will reduce this fraction. The
composition, small size, highly elongated shape, and tumbling motion of
`Oumuamua is consistent with ISAs generated by misaligned CBDs.
