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We present results on the star cluster properties from a series of highresolution smoothed particles hydrodynamics (SPH) simulations of isolated dwarfgalaxies as part of the GRIFFIN project. The simulations at sub-parsec spatialresolution and a minimum particle mass of 4 $\mathrm{M_\odot}$ incorporatenon-equilibrium heating, cooling and chemistry processes, and realiseindividual massive stars. All the simulations follow feedback channels ofmassive stars that include the interstellar-radiation field, that is variablein space and time, the radiation input by photo-ionisation and supernovaexplosions. Varying the star formation efficiency per free-fall time in therange $\epsilon_\mathrm{ff}$ = 0.2 - 50$\%$ neither changes the star formationrates nor the outflow rates. While the environmental densities at starformation change significantly with $\epsilon_\mathrm{ff}$, the ambientdensities of supernovae are independent of $\epsilon_\mathrm{ff}$ indicating adecoupling of the two processes. At low $\epsilon_\mathrm{ff}$, more massive,and increasingly more bound star clusters are formed, which are typically notdestroyed. With increasing $\epsilon_\mathrm{ff}$ there is a trend forshallower cluster mass functions and the cluster formation efficiency $\Gamma$for young bound clusters decreases from $50 \%$ to $\sim 1 \%$ showing evidencefor cluster disruption. However, none of our simulations form low mass ($<10^3$ $\mathrm{M_\odot}$) clusters with structural properties in perfectagreement with observations. Traditional star formation models used in galaxyformation simulations based on local free-fall times might therefore not beable to capture low mass star cluster properties without significantfine-tuning.

The challenge of simulating the star cluster population of dwarf galaxies with resolved interstellar medium