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 .