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tokens: that R 90 is highly dependent on the finding algorithm. Interacting galaxies show a very wide f Y distribution for all quantities studied. There is an evident difference between host and satellite galaxies, which peak at f Y > 1 and f Y 1, respectively. These differences are mainly caused by inadequate particle assignment in halomaker , which we show our improved version of velociraptor handles better. halomaker artificially increases (decreases) the estimated values of M * , SFR, and R 50,90 for host (satellite) galaxies in interacting systems. Differences between the catalogues are amplified at higher redshifts, where the f Y distributions of interacting and isolated galaxies widen. Galaxy population statistics . We investigate how the choice of finder affects the overall galaxy population statistics. We explore the GSMF, SFRF, and mass–size relation for R 50 and R 90 . At M * 10 11 M ⊙ the z = 0 GSMFs of halomaker and velociraptor agree well, while at higher stellar masses the former predicts from 20 per cent to 100 per cent more galaxies than the latter. At higher redshifts differences are amplified. At z = 4 halomaker ’s GSMF predicts a number density of galaxies at least 30 per cent higher than that of velociraptor over the whole mass range, increasing to 100 per cent at M * ≳ 10 10 M ⊙ . The SFRF at z = 0 is also fairly similar between the finders, with differences increasing with redshift. At z = 2, the peak of the cosmic star formation history, halomaker predicts up to 50 per cent more galaxies at than velociraptor . This is important as these galaxies are expected to dominate the cosmic SFR. We compare the R 50 and R 90 size–mass relation predicted by both finders. We find that the R 50 mass–size relations resulting from the two finders are similar, except at the high-mass end, M * ≃ 10 12 M ⊙ , where halomaker’s galaxies are 20 per cent larger than velociraptor’s . These differences increase by 30 per cent when we study R 90 . This results from the fact that the stellar content and structure in the outskirts of galaxies are very sensitive to the choice of finder. Although we see that the overall z = 0 galaxy statistics are not greatly impacted by the choice of finder, individual galaxies can display differences in mass and size of more than a factor of 3 between the two finders studied here. We suggest that the tuning of simulations of galaxy formation is relatively robust as it has consistently focused on population statistics. However, comparisons of galaxy subpopulations with observations, specifically in the context of pairs, groups, and clusters, can be greatly affected by the choice of finder. We showed that our new algorithm outperforms 3D finders and provides extensive evidence of this. One of our key findings is that the stellar outskirts of galaxies is greatly affected by the choice of finder. In upcoming studies we will explore in detail the diffuse IHSC, the stellar streams, and the outer stellar profiles of