  Many fundamental physical processes regarding planetary formation in
protoplanetary disks are still imperfectly understood, with an elusive
phenomenon being turbulence in such disks. Observations are available of
planetary systems and of some protoplanetary disks, which can serve as a
starting point for these investigations. Detected systems reveal different
architectures of planets. One particularly interesting case to consider is the
Kepler-223 system, which contains a rare configuration of four planets in a
resonance chain, implying a certain migration history. We aim to use the
orbital configuration of Kepler-223's planets to constrain the parameters of
the protoplanetary disk that allow for the formation of a chain of mean-motion
resonances that resembles the one of Kepler-223. The parameters we aim to
investigate are primarily the disk viscosity and surface density. We use the
swift_symba N-body integrator with additional dissipative forces to mimic
planet-disk interactions. We constrain the surface densities and viscosities
that allow the formation of a resonant chain like that of Kepler-223. We find
that surface densities of up to a few minimum mass solar nebula (MMSN) surface
densities and disk viscosity parameters $\alpha$ of a few $10^{-3}$ up to
$10^{-2}$ are most successful at reproducing the architecture of this
particular planetary system. We describe how these two quantities are linked to
each other considering the success of reproducing the chain and find that
higher disk surface densities in turn require lower viscosities to build the
chain. Our results show that well characterized observed planetary systems hold
information about their formation conditions in the protoplanetary disks and
that it is possible to extract this information, namely the initial disk
surface density and viscosity, helping to constrain planet formation.
