  Using resistive magnetohydrodynamics simulations, the propagation of
protostellar jets, the formation of circumstellar discs and the configuration
of magnetic fields are investigated from the prestellar cloud phase until
$\sim$500 yr after protostar formation. As the initial state, we prepare
magnetized rotating clouds, in which the rotation axis is misaligned with the
global magnetic field by an angle $\theta_0$. We calculate the cloud evolution
for nine models with different $\theta_0 (=$ 0, 5, 10, 30, 45, 60, 80, 85,
90$^\circ$). Our simulations show that there is no significant difference in
the physical quantities of the protostellar jet, such as the mass and momentum,
among the models except for the model with $\theta_0=90^\circ$. On the other
hand, the directions of the jet, disc normal and magnetic field are never
aligned with each other during the early phase of star formation except for the
model with $\theta_0=0^\circ$. Even when the rotation axis of the prestellar
cloud is slightly inclined to the global magnetic field, the directions of the
jet, disc normal and local magnetic field differ considerably, and they
randomly change over time. Our results indicate that it is very difficult to
extract any information from the observations of the directions of the outflow,
disc and magnetic field at the scale of $\lesssim 1000$ au. Thus, we cannot use
such observations to derive any restrictions on the star formation process.
