  Galaxy clusters are known to induce gas loss in infalling galaxies due to the
ram pressure exerted by the intracluster medium over their gas content. In this
paper, we investigate this process through a set of simulations of Milky Way
like galaxies falling inside idealised clusters of 10$^{14}$ M$_\odot$ and
10$^{15}$ M$_\odot$, containing a cool-core or not, using the adaptive mesh
refinement code RAMSES. We use these simulations to constrain how much of the
initial mass contained in the gaseous disk of the galaxy will be converted into
stars and how much of it will be lost, after a single crossing of the entire
cluster. We find that, if the galaxy reaches the central region of a cool-core
cluster, it is expected to lose all its gas, independently of its entry
conditions and of the cluster's mass. On the other hand, it is expected to
never lose all its gas after crossing a cluster without a cool-core just once.
Before reaching the centre of the cluster, the SFR of the galaxy is always
enhanced, by a factor of 1.5 to 3. If the galaxy crosses the cluster without
being completely stripped, its final amount of gas is on average two times
smaller after crossing the 10$^{15}$ M$_\odot$ cluster, relative to the
10$^{14}$ M$_\odot$ cluster. This is reflected in the final SFR of the galaxy,
which is also two times smaller in the former, ranging from 0.5 $-$ 1 M$_\odot$
yr$^{-1}$, compared to 1 $-$ 2 M$_\odot$ yr$^{-1}$ for the latter.
