  Binary stars play a major role in determining the dynamic evolution of star
clusters. We used images collected with the Hubble Space Telescope to study
fourteen Magellanic Clouds star clusters that span an age interval between
$\sim 0.6$ and $2.1$ Gyr and masses of $10^{4}-10^{5}$ M$_{\odot}$. We
estimated the fraction of binary systems composed of two main-sequence stars
and the fraction of candidate blue-straggler stars (BSSs). Moreover, we derived
the structural parameters of the cluster, including the core radius, the
central density, the mass function, and the total mass. We find that the
fraction of binaries with a mass ratio larger than 0.7 ranges from $\sim$7%, in
NGC1846, to $\sim$20%, in NGC2108. The radial and luminosity distribution can
change from one cluster to another. However, when we combine the results from
all the clusters, we find that binaries follow a flat radial trend and no
significant correlation with the mass of the primary star. We find no evidence
for a relation between the fractions of binaries and BSSs. We combined the
results on binaries in the studied Magellanic Cloud clusters with those
obtained for 67 Galactic globular clusters and 78 open clusters. We detect a
significant anti-correlation between the binary fraction in the core and the
mass of the host cluster. However, star clusters with similar masses exhibit a
wide range of binary fractions. Conversely, there is no evidence of a
correlation between the fraction of binaries and either the cluster age or the
dynamic age.
