  We use a newly developed cascade model of turbulent concentration of
particles in protoplanetary nebulae to calculate several properties of interest
to the formation of primitive planetesimals and to the meteorite record. The
model follows, and corrects, calculations of the primary planetesimal Initial
Mass Function (IMF) by Cuzzi et al. (2010), in which an incorrect cascade model
was used. Here we use the model of Hartlep et al. (2017), which has been
validated against several published numerical simulations of particle
concentration in turbulence. We find that, for a range of nebula and particle
properties, planetesimals may be "born big", formed as sandpiles with diameters
in the 10-100 km range, directly from freely floating particles. The IMFs have
a modal nature, with a well-defined peak rather than a powerlaw size
dependence. Predictions for the inner and outer nebula behave similarly in
these regards, and observations of inner and outer nebula primitive bodies
support such modal IMFs. Also, we present predictions of local particle
concentrations on several lengthscales in which particles "commonly" find
themselves, which have significance for meteoritical observations of the redox
state and isotopic fractionation in regions of chondrule formation. An
important difference between these results, and those of Cuzzi et al. (2010),
is that particle growth-by-sticking must proceed to at least the 1-few cm
radius range for the IMF and meteoritical properties to be most plausibly
satisfied. That is, as far as the inner nebula goes, the predominant
"particles" must be aggregates of chondrules (or chondrule-size precursors)
rather than individual chondrules themselves.
