Circumstellar discs are the precursors of planetary systems and develop shortly after their host star has formed .
In their early stages these discs are immersed in an environment rich in gas and neighbouring stars , which can be hostile for their survival .
There are several environmental processes that can affect the evolution of circumstellar discs , and external photoevaporation is arguably one of the most important ones .
Theoretical and observational evidence point to circumstellar discs losing mass quickly when in the vicinity of massive , bright stars .
External photoevaporation can then constrain the time and material available to form planets .
The stellar density of the region seems to influence the extent of the effects of external photoevaporation .
In this work we perform simulations of star clusters with a range of stellar densities .
Stars with masses \mathrm { M } _ { * } \leq 1.9 \mathrm { M } _ { \odot } \mathrm { } are surrounded by a disc , and stars with masses \mathrm { M } _ { * } > 1.9 \mathrm { M } _ { \odot } \mathrm { } are considered as emitting radiation .
Our results show that external photoevaporation is efficient in depleting disc masses and that the degree of its effect is related to stellar density .
Dense clusters have \sim 10 \% surviving discs by \SI { 2 } { Myr } , whereas sparse ones have \sim 50 \% .
Surviving discs in sparser regions also span a larger range of masses .
We compare our results to observations of the Lupus clouds , the Orion Nebula Cluster , the Orion Molecular Cloud-2 , Taurus , and NGC 2024 , and find that the trends observed between region density and disc masses are similar to those in our simulations .