  The star-forming clumps in star-bursting dwarf galaxies provide valuable
insights into the understanding of the evolution of dwarf galaxies. In this
paper, we focus on five star-bursting dwarf galaxies featuring off-centered
clumps in the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA)
survey. Using the stellar population synthesis software FADO, we obtain the
spatially-resolved distribution of the star formation history, which allows us
to construct the $g$-band images of the five galaxies at different ages. These
images can help us to probe the evolution of the morphological structures of
these galaxies. While images of stellar population older than 1 Gyr are
typically smooth, images of stellar population younger than 1 Gyr reveal
significant clumps, including multiple clumps which appear at different
locations and even different ages. To study the evolutionary connections of
these five galaxies to other dwarf galaxies before their star-forming clumps
appear, we construct the images of the stellar populations older than three age
nodes, and define them to be the images of the "host" galaxies. We find that
the properties such as the central surface brightness and the effective radii
of the hosts of the five galaxies are in between those of dwarf ellipticals
(dEs) and dwarf irregulars (dIrrs), with two clearly more similar to dEs and
one more similar to dIrrs. Among the five galaxies, 8257-3704 is particularly
interesting, as it shows a previous starburst event that is not quite visible
from its $gri$ image, but only visible from images of the stellar population at
a few hundred million years. The star-forming clump associated with this event
may have appeared at around 600 Myr and disappeared at around 40 Myr.
