  If planetesimal formation is an efficient process, as suggested by several
models involving gravitational collapse of pebble clouds, then, before long, a
significant part of the primordial dust mass should be absorbed in many km
sized objects. A good understanding of the total amount of solids in the disk
around a young star is crucial for planet formation theory. But as the mass of
particles above the mm size cannot be assessed observationally, one must ask
how much mass is hidden in bigger objects. We perform 0-d local simulations to
study how the planetesimal to dust and pebble ratio is evolving in time and to
develop an understanding of the potentially existing mass in planetesimals for
a certain amount of dust and pebbles at a given disk age. We perform a
parameter study based on a model considering dust growth, planetesimal
formation and collisional fragmentation of planetesimals, while neglecting
radial transport processes. While at early times, dust is the dominant solid
particle species, there is a phase during which planetesimals make up a
significant portion of the total mass starting at approximately $10^4 - 10^6$
yr. The time of this phase and the maximal total planetesimal mass strongly
depend on the distance to the star $R$, the initial disk mass, and the
efficiency of planetesimal formation $\epsilon$. After approximately $10^6$ yr,
our model predicts planetesimal collisions to dominate, which resupplies small
particles. In our model, planetesimals form fast and everywhere in the disk.
For a given $\epsilon$, we were able to relate the dust content and mass of a
given disk to its planetesimal content, providing us with some helpful basic
intuition about mass distribution of solids and its dependence on underlying
physical processes.
