  Here we present new ALMA observations of polarized dust emission from six of
the most massive clumps in W43-Main. The clumps MM2, MM3, MM4, MM6, MM7, and
MM8, have been resolved into two populations of fragmented filaments. From
these two populations we extracted 81 cores (96 with the MM1 cores) with masses
between 0.9 \Msun\ to 425 \Msun\ and a mass sensitivity of 0.08 M$_{\odot}$.
The MM6, MM7, and MM8 clumps show significant fragmentation, but the polarized
intensity appears to be sparse and compact. The MM2, MM3, and MM4 population
shows less fragmentation, but with a single proto-stellar core dominating the
emission at each clump. Also, the polarized intensity is more extended and
significantly stronger in this population. From the polarized emission, we
derived detailed magnetic field patterns throughout the filaments which we used
to estimate field strengths for 4 out of the 6 clumps. The average field
strengths estimations were found between 500 $\mu$G to 1.8 mG. Additionally, we
detected and modeled infalling motions towards MM2 and MM3 from single dish
HCO$^{+}(J=4 \rightarrow 3)$ and HCN$(J=4 \rightarrow 3)$ data resulting in
mass infall rates of $\dot{\mathrm{M}}_{\mathrm{MM2}} = 1.2 \times 10^{-2}$
\Msun\ yr$^{-1}$ and $\dot{\mathrm{M}}_{\mathrm{MM3}} = 6.3 \times 10^{-3}$
\Msun\ yr$^{-1}$. By using our estimations, we evaluated the dynamical
equilibrium of our cores by computing the total virial parameter
$\alpha_{\mathrm{total}}$. For the cores with reliable field estimations, we
found that 71\% of them appear to be gravitationally bound while the remaining
29\% are not. We concluded that these unbound cores, also less massive, are
still accreting and have not yet reached a critical mass. This also implies
different evolutionary time-scales, which essentially suggests that
star-formation in high mass filaments is not uniform.
