  Most of massive stars form in binary or higher-order systems in clumpy,
sub-structured clusters. In the very first phases of their life, these stars
are expected to interact with the surrounding environment, before being
released to the field when the cluster is tidally disrupted by the host galaxy.
We present a set of N-body simulations to describe the evolution of young
stellar clusters and their binary content in the first phases of their life. To
do this, we have developed a method that generates realistic initial conditions
for binary stars in star clusters from hydrodynamical simulations. We
considered different evolutionary cases to quantify the impact of binary and
stellar evolution. Also, we compared their evolution to that of King and
fractal models with different length scales. Our results indicate that the
global expansion of the cluster from hydrodynamical simulations is initially
balanced by the sub-clump motion and accelerates when a monolithic shape is
reached, as in a post-core collapse evolution. Compared to the spherical
initial conditions, the ratio of the 50% to 10% Lagrangian radius shows a very
distinctive trend, explained by the formation of a hot core of massive stars
triggered by the high initial degree of mass segregation. As for its binary
population, each cluster shows a self-regulating behaviour by creating
interacting binaries with binding energies of the order of its energy scales.
Also, in absence of original binaries, the dynamically formed binaries present
a mass dependent binary fraction, that mimics the trend of the observed one.
