  More and more observations indicate that young star clusters could retain
imprints of their formation process. In particular, the degree of
substructuring and rotation are possibly the direct result of the collapse of
the parent molecular cloud from which these systems form. Such properties can,
in principle, be washed-out, but they are also expected to have an impact on
the relaxation of these systems. We ran and analyzed a set of ten
hydrodynamical simulations of the formation of embedded star clusters through
the collapse of turbulent massive molecular clouds. We systematically studied
the fractality of our star clusters, showing that they are all extremely
substructured (fractal dimension $D=1.0-1.8$). We also found that fractality is
slowly reduced, with time, on small scales, while it persists on large scales
on longer timescales. Signatures of rotation are found in different simulations
at every time of the evolution, even for slightly supervirial substructures,
proving that the parent molecular gas transfers part of its angular momentum to
the new stellar systems.
