  We take into account redshift-space distortion measurements to investigate
the growth of cosmological large-scale structures within the framework of
modified symmetric teleparallel $f(Q)$ gravity. After comparing the predictions
of the $f(Q)$-gravity expansion history with OHD and SNIa datasets and
constraining the pertinent cosmological parameters $\Omega_{m}$ and $H_0$,
together with the exponent $n$ for $f(Q)$ power-law models, we derive the full
system of equations governing linear cosmological perturbations to study matter
fluctuations using the $1 + 3$ covariant formalism when applied to $f(Q)$
gravity. Thus, we resort to both the usual redshift-space distortion data
$f\sigma_8$ and some recent separate measurements of the growth rate $f$ and
the amplitude of matter fluctuations $\sigma_8$ from the VIPERS and SDSS
collaborations to find the best-fit cosmological parameters $\Omega_m$,
$\sigma_{8}$ and $n$. We also apply a collective analysis of such
growth-structure data together with the aforementioned cosmic expansion
measurements, to restrict these parameters through Monte Carlo Markov Chain
simulations. determining the statistical significance for the best-fit
parameter values through the AIC and BIC Bayesian selection criteria.
