  Many galaxy clusters show diffuse cluster-scale emission in the form of radio
halos, showing that magnetic fields and relativistic electrons are mixed in
with the intra-cluster medium (ICM). There is general agreement that the origin
of radio halos is connected to turbulence, generated during cluster mergers.
Statistical studies of large samples of galaxy clusters in the radio band have
the potential to unveil the connection between the properties of radio halos
and the mass and dynamics of the host clusters. Previous studies have been
limited to massive clusters and based on a small number of radio halos. The aim
of this paper is to investigate the scaling relation between the radio power of
radio halos and the mass of the host clusters at low frequencies and down to
lower cluster masses. We analysed the clusters from the second catalogue of
Planck Sunyaev Zel'dovich sources that lie within the 5634 sq deg covered by
the second Data Release of the LOFAR Two-meter Sky Survey. We derived the
correlation between the radio power and the mass of the host clusters and we
investigated the distribution of clusters without radio halos with respect to
the correlation. We use X-ray observations to classify the dynamical state of
clusters and investigate its role on the power of radio halos. We found a
correlation between the power of radio halos at 150 MHz and the mass of the
host clusters down to 3e14 Msun. This correlation has a large scatter, part of
which can be attributed to the different dynamical states of host clusters. We
used two statistical test to show that the distribution of clusters with and
without (upper limits) radio halos in the mass-radio power diagram is not
compatible with a single correlation and that it is also not compatible with
clusters being uniformly distributed below an upper envelope constituted by the
correlation.
