  We present in this paper a detailed study of the kinematical properties of
the ionized gas around the young massive star clusters in the nucleus of NGC
4214. The analysis is based on bidimensional spectroscopical data, allowing to
derive the spatial variation of different properties (intensity, velocity and
width / line splitting) of the emission lines H\alpha and [O III] \lambda 5007
along the nuclear region. We have found that the Giant H II region around the
two most massive clusters in NGC 4214 (A and B) is resolved into two clearly
separated regions. We have not detected superbubbles with the properties we
would expect according to the evolutionary state of the stellar clusters, but
just a partial ring feature around the most massive one and two expanding
shells around cluster B. The first expanding shell seems to have experienced
blowout, whereas the second one is still complete. A possible explanation to
this phenomenon is that the most massive stars in a starburst spend a large
fraction of their lives buried inside their original molecular clouds.
Champagne flows might have formed at the borders of the regions, especially on
the SE complex, explaining the existence of the diffuse ionized gas around the
galaxy. As a consequence of these results we postulate that NGC 4214 is indeed
a dwarf spiral galaxy, with a thin (around 200 pc) disk that inhibits the
formation of large scale structures in the ISM. The mechanical input deposited
by the star formation complexes, in a variety of physical processes that
include the free expanding bubbles liberated after blowout and photoevaporation
of the parent clouds, have succeeded in generating the structures now detected
far from the disk, giving place to the large-scale structure which now enriches
the optical appearance of the galaxy.
