  We conducted isothermal MHD simulations with self-gravity to investigate the
properties of dense cores in cluster-forming clumps. Two different setups were
explored: a single rotating clump and colliding clumps. We focused on
determining the extent to which the formed dense cores inherit the rotation and
magnetic field of the parental clump. Our statistical analysis revealed that
the alignment between the angular momentum of dense cores, $\bf{L}_{\rm core}$,
and the rotational axis of the clump is influenced by the strength of
turbulence and the simulation setup. In single rotating clumps, we found that
$\bf{L}_{\rm core}$ tends to align with the clump's rotational axis if the
initial turbulence is weak. However, in colliding clumps, this alignment does
not occur, regardless of the initial turbulence strength. This misalignment in
colliding clumps is due to the induced turbulence from the collision and the
isotropic gas inflow into dense cores. Our analysis of colliding clumps also
revealed that the magnetic field globally bends along the shock-compressed
layer, and the mean magnetic field of dense cores, $\bf{B}_{\rm core}$, aligns
with it. Both in single rotating clumps and colliding clumps, we found that the
angle between $\bf{B}_{\rm core}$ and $\bf{L}_{\rm core}$ is generally random,
regardless of the clump properties. We also analyzed the dynamical states of
the formed cores and found a higher proportion of unbound cores in colliding
clumps. In addition, the contribution of rotational energy was only
approximately 5% of the gravitational energy, regardless of the model
parameters for both single and colliding cases.
