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Aims. Dust plays a crucial role in the evolution of protoplanetary disks. Westudy the dynamics and growth of initially sub-$\mu m$ dust particles inself-gravitating young protoplanetary disks with various strengths of turbulentviscosity. We aim to understand the physical conditions that determine theformation and spatial distribution of pebbles when both disk self-gravity andturbulent viscosity can be concurrently at work. Methods. We perform thethin-disk hydrodynamics simulations of self-gravitating protoplanetary disksover an initial time period of 0.5 Myr using the FEOSAD code. Turbulentviscosity is parameterized in terms of the spatially and temporally constant$\alpha$-parameter, while the effects of gravitational instability on dustgrowth is accounted for by calculating the effective parameter $\alpha_{\rmGI}$. We consider the evolution of dust component including momentum exchangewith gas, dust self-gravity, and also a simplified model of dust growth.Results. We find that the level of turbulent viscosity strongly affects thespatial distribution and total mass of pebbles in the disk. The$\alpha=10^{-2}$ model is viscosity-dominated, pebbles are completely absent,and dust-to-gas mass ratio deviates from the reference 1:100 value no more thanby 30\% throughout the disk extent. On the contrary, the $\alpha=10^{-3}$ modeland, especially, the $\alpha=10^{-4}$ model are dominated by gravitationalinstability. The effective parameter $\alpha+\alpha_{\rm GI}$ is now a stronglyvarying function of radial distance. As a consequence, a bottle neck effectdevelops in the innermost disk regions, which makes gas and dust accumulate ina ring-like structure. Abridged.

Formation of pebbles in (gravito-)viscous protoplanetary disks with various turbulent strengths