  We present a calculation of protostellar disk formation and evolution in
which gaseous clumps (essentially, the first Larson cores formed via disk
fragmentation) are ejected from the disk during the early stage of evolution.
This is a universal process related to the phenomenon of ejection in multiple
systems of point masses. However, it occurs in our model entirely due to the
interaction of compact, gravitationally-bound gaseous clumps and is free from
the smoothing-length uncertainty that is characteristic of models using sink
particles. Clumps that survive ejection span a mass range of 0.08--0.35
$M_\odot$, and have ejection velocities $0.8 \pm 0.35$ km s$^{-1}$, which are
several times greater than the escape speed. We suggest that, upon contraction,
these clumps can form substellar or low-mass stellar objects with notable
disks, or even close-separation very-low-mass binaries. In this hybrid
scenario, allowing for ejection of clumps rather than finished
protostars/proto--brown-dwarfs, disk formation and the low velocity dispersion
of low-mass objects are naturally explained, while it is also consistent with
the observation of isolated low-mass clumps that are ejection products. We
conclude that clump ejection and the formation of isolated low mass stellar and
substellar objects is a common occurrence, with important implications for
understanding the initial mass function, the brown dwarf desert, and the
formation of stars in all environments and epochs.
