  The amount of turbulent pressure in galaxy clusters is still debated,
especially as for the impact of the dynamical state and the hydro-method used
for simulations. We study the turbulent pressure fraction in the intra cluster
medium of massive galaxy clusters. We aim to understand the impact of the
hydrodynamical scheme, analysis method, and dynamical state on the final
properties of galaxy clusters from cosmological simulations. We perform
non-radiative simulations of a set of zoom-in regions of seven galaxy clusters
with Meshless Finite Mass (MFM) and Smoothed Particle Hydrodynamics (SPH). We
use three different analysis methods based on: $(i)$ the deviation from
hydrostatic equilibrium, $(ii)$ the solenoidal velocity component obtained by a
Helmholtz-Hodge decomposition, and $(iii)$ the small-scale velocity obtained
through a multi-scale filtering approach. We split the sample of simulated
clusters into active and relaxed clusters. Our simulations predict an increased
turbulent pressure fraction for active compared to relaxed clusters. This is
especially visible for the velocity-based methods. For these, we also find
increased turbulence for the MFM simulations compared to SPH, consistent with
findings from more idealized simulations. The predicted non-thermal pressure
fraction varies between a few percent for relaxed clusters and $\approx13\%$
for active ones within the cluster center and increases towards the outskirts.
No clear trend with redshift is visible. Our analysis quantitatively assesses
the importance played by the hydrodynamical scheme and the analysis method to
determine the non-thermal/turbulent pressure fraction. While our setup is
relatively simple (non-radiative runs), our simulations show agreement with
previous, more idealized simulations, and make a step further toward the
understanding of turbulence.
