We examine the properties of the galaxies and dark matter haloes residing in the cluster infall region surrounding the simulated $\Lambda$ cold dark matter galaxy cluster studied by Elahi et al. at $z$ = 0. The 1.1 × 10$\mathrm{<mrow\; data-mjx-texclass="ORD">15</mrow>}$ $h-1$ M$\odot$ galaxy cluster has been simulated with eight different hydrodynamical codes containing a variety of hydrodynamic solvers and sub-grid schemes. All models completed a dark-matter-only, non-radiative and full-physics run from the same initial conditions. The simulations contain dark matter and gas with mass resolution $mDM$ = 9.01 × 10$8$ $h-1$ M$\odot$ and $mgas$ = 1.9 × 10$8$ $h-1$ M$\odot$, respectively. We find that the synthetic cluster is surrounded by clear filamentary structures that contain ~60 per cent of haloes in the infall region with mass ~10$\mathrm{<mrow\; data-mjx-texclass="ORD">12.5</mrow>}$–10$\mathrm{<mrow\; data-mjx-texclass="ORD">14</mrow>}$ $h-1$ M$\odot$, including 2–3 group-sized haloes (>10$\mathrm{<mrow\; data-mjx-texclass="ORD">13</mrow>}$ $h-1$ M$\odot$). However, we find that only ~10 per cent of objects in the infall region are sub-haloes residing in haloes, which may suggest that there is not much ongoing pre-processing occurring in the infall region at $z$ = 0. By examining the baryonic content contained within the haloes, we also show that the code-to-code scatter in stellar fraction across all halo masses is typically ~2 orders of magnitude between the two most extreme cases, and this is predominantly due to the differences in sub-grid schemes and calibration procedures that each model uses. Models that do not include active galactic nucleus feedback typically produce too high stellar fractions compared to observations by at least ~1 order of magnitude.