  In this paper we further advance the study of magnetic field amplification in
the interstellar medium that was started in Balsara et al (2004, Paper I). We
show that the flux growth rate is comparable to the rate of magnetic energy
growth found in Paper I. We also demonstrate the role of intermittency in field
amplification. The density shows a double-peaked PDF, consistent with the
cooling curve that was used. The PDF of the magnetic field shows a high-end
tail, providing a tell-tale signature of the operation of the small scale
dynamo. The magnetic field strength correlates positively with the density. As
a result, the field amplification takes place more vigorously in the lower
temperature, denser gas. The Lagrangian chaos in the simulated turbulent flows
is studied in substantial detail. It is shown that the stretching rate of
material lines as well as the Lyapunov exponents can be used to gain important
insights into the growth of magnetic field. The cancellation exponent for the
small scale supernova-driven dynamo is derived and it is shown that
constructive folding of field lines in the dynamo is very inefficient. We also
show that our Lagrangian approach can yield actual measures of the turbulent
diffusivity in the simulated ISM. The turbulent diffusivity provides insights
into the mixing of elements from supernova ejecta on macroscopic scales. The
high rates of line stretching in interstellar turbulence suggests that the
eventual diffusion of elements at the molecular level is very efficient. Many
of the diagnostics of turbulence that are presented here can be used to make
direct connections between simulations and observations.
