  Several lines of evidence suggest that protogalactic and galactic
environments manage to grow magnetic field very rapidly. This makes the
theoretical problem of achieving rapid growth of magnetic fields in such
environments difficult. Following Balsara, Benjamin and Cox (2001), we show
that a multiphase ISM that is dominated by realistic energy inputs via
supernova explosions will naturally become a strongly turbulent medium with
large positive and negative values of the fluid helicity. The resultant
interstellar turbulence seems to have some of the essential characteristics of
a fast dynamo. Magnetic field growth in such a turbulent dynamo is studied in
this paper. It is shown that the field undergoes a linear phase of evolution
where it has a time of growth that is comparable to the eddy turn-over time.
Energetics, power spectra, statistics and structures of the turbulent dynamo
are studied here. It is shown that despite the fact that the ISM is driven by
compressive motions, the kinetic energy in this high Mach number flow is mainly
concentrated in solenoidal motions rather than compressive motions.
