  We investigate the impact of turbulence on magnetic reconnection through
high-resolution 3D MHD simulations, covering Lundquist numbers from $S=10^3$ to
$10^6$. Our simulations introduce small-scale perturbations injected into the
system until $t=0.1\, t_A$. Even after the initial perturbation ceases,
turbulence grows and persists, leading to sustained high reconnection rates of
$V_\text{rec}/V_A \sim 0.03-0.08$, which surpass those generated solely by
resistive tearing modes (plasmoids) observed in 2D and 3D PIC/MHD simulations
by factors of 5 to 6. Our findings reveal that the achieved reconnection rates
align with observations in solar phenomena and those reported in 3D MHD global
simulations of accretion flows and relativistic jets. Notably, our simulations
exhibit a steady-state reconnection rate coinciding with the full development
of turbulence, showcasing the robustness and persistence of the reconnection in
a turbulent environment. We establish the independence of the reconnection rate
from the Lundquist number, consistent with the theory of turbulent reconnection
proposed by Lazarian and Vishniac. Our results demonstrate a mild dependence of
$V_\text{rec}$ on the plasma-$\beta$ parameter, the ratio between the thermal
and magnetic pressure, illustrating a decrease from $0.036$ to $0.028$ as
$\beta$ increases from $2$ to $64$ for simulations with $S=10^5$. Finally, we
explore the influence of the magnetic Prandtl number ($\text{Pr}_m=\nu/\eta$)
on the reconnection rate and find this influence to be negligible during the
turbulent regime across the range tested, from $\text{Pr}_m=1$ to $60$. These
findings carry significant implications for research into reconnection and
particle acceleration within realistic magnetized space and astrophysical
environments.
