  We investigate the formation and evolution of "primordial" dusty rings
occurring in the inner regions of protoplanetary discs, with the help of
long-term, coupled dust-gas, magnetohydrodynamic simulations. The simulations
are global and start from the collapse phase of the parent cloud core, while
the dead zone is calculated via an adaptive $\alpha$ formulation by taking into
account the local ionization balance. The evolution of the dusty component
includes its growth and back reaction on to the gas. Previously, using
simulations with only a gas component, we showed that dynamical rings form at
the inner edge of the dead zone. We find that when dust evolution as well as
magnetic field evolution in the flux-freezing limit are included, the dusty
rings formed are more numerous and span a larger radial extent in the inner
disc, while the dead zone is more robust and persists for a much longer time.
We show that these dynamical rings concentrate enough dust mass to become
streaming unstable, which should result in rapid planetesimal formation even in
the embedded phases of the system. The episodic outbursts caused by the
magnetorotational instability have significant impact on the evolution of the
rings. The outbursts drain the inner disc of grown dust, however, the period
between bursts is sufficiently long for the planetesimal growth via streaming
instability.The dust mass contained within the rings is large enough to
ultimately produce planetary systems with the core accretion scenario. The low
mass systems rarely undergo outbursts and thus, the conditions around such
stars can be especially conducive for planet formation.
