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Galaxy clusters are known to induce gas loss in infalling galaxies due to theram pressure exerted by the intracluster medium over their gas content. In thispaper, we investigate this process through a set of simulations of Milky Waylike galaxies falling inside idealised clusters of 10$^{14}$ M$_\odot$ and10$^{15}$ M$_\odot$, containing a cool-core or not, using the adaptive meshrefinement code RAMSES. We use these simulations to constrain how much of theinitial mass contained in the gaseous disk of the galaxy will be converted intostars and how much of it will be lost, after a single crossing of the entirecluster. We find that, if the galaxy reaches the central region of a cool-corecluster, it is expected to lose all its gas, independently of its entryconditions and of the cluster's mass. On the other hand, it is expected tonever 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 alwaysenhanced, by a factor of 1.5 to 3. If the galaxy crosses the cluster withoutbeing completely stripped, its final amount of gas is on average two timessmaller after crossing the 10$^{15}$ M$_\odot$ cluster, relative to the10$^{14}$ 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.

The fate of the gaseous disks of galaxies that fall into clusters