We show that in clustering dark energy models the growth index of linear matter perturbations, $gamma$, can be much lower than in $Lambda$CDM or smooth quintessence models and present a strong variation with redshift. We find that the impact of dark energy perturbations on $gamma$ is enhanced if the dark energy equation of state has a large and rapid decay at low redshift. We study four different models with these features and show that we may have $0.33<gammaleft(zright)<0.48$ at $0<z<3$. We also show that the constant $gamma$ parametrization for the growth rate, $f=dlndelta_{m}/dln a=Omega_{m}^{gamma}$, is a few percent inaccurate for such models and that a redshift dependent parametrization for $gamma$ can provide about four times more accurate fits for $f$. We discuss the robustness of the growth index to distinguish between General Relativity with clustering dark energy and modified gravity models, finding that some $fleft(Rright)$ and clustering dark energy models can present similar values for $gamma$.
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