  The diffuse very high-energy (VHE, > 100 GeV) gamma-ray emission observed in
the central 200 pc of the Milky Way by H.E.S.S. was found to follow the dense
matter distribution in the Central Molecular Zone (CMZ) up to a longitudinal
distance of about 130 pc to the Galactic Centre (GC), where the flux rapidly
decreases. Recent sensitive H.E.S.S. analysis revealed that the cosmic-ray (CR)
density profile drops with the distance to the centre, making data compatible
with a steady cosmic PeVatron at the GC. In this paper, we extend this analysis
to obtain for the first time a detailed characterisation of the correlation
with matter and to search for additional features and individual gamma-ray
sources in the inner 200 pc. Taking advantage of 250 hours of H.E.S.S. data and
improved analysis techniques we perform a detailed morphology study of the
diffuse VHE emission observed from the GC ridge and reconstruct its total
spectrum. We show that the emission correlated with dense matter covers the
full CMZ and that its flux is about half the total diffuse emission flux. We
also detect some emission at higher latitude likely produced by hadronic
collisions of CRs in less dense regions of the GC interstellar medium. We
detect an additional emission component centred on the GC and extending over
about 15 pc that is consistent with the existence of a strong CR density
gradient and confirms the presence of a CR accelerator at the very centre of
our Galaxy. We show that the spectrum of the full ridge diffuse emission is
compatible with the one previously derived from the central regions, suggesting
that a single population of particles fills the entire CMZ. Finally, we report
the discovery of a VHE gamma-ray source near the GC radio arc and argue that it
is produced by the pulsar wind nebula candidate G0.13-0.11.
