  The strongly coupled hydrodynamic, magnetic, and radiation properties of the
plasma in the solar chromosphere makes it a region of the Sun's atmosphere that
is poorly understood. We use data obtained with the high-resolution Visible
Broadband Imager (VBI) equipped with an H$\beta$ filter and the Visible
Spectro-Polarimeter (ViSP) at the Daniel K. Inouye Solar Telescope to
investigate the fine-scale structure of the plage chromosphere. To aid the
interpretation of the VBI imaging data, we also analyze spectra from the
CHROMospheric Imaging Spectrometer on the Swedish Solar Telescope. The analysis
of spectral properties, such as enhanced line widths and line depths explains
the high contrast of the fibrils relative to the background atmosphere
demonstrating that H$\beta$ is an excellent diagnostic for the enigmatic
fine-scale structure of the chromosphere. A correlation between the parameters
of the H$\beta$ line indicates that opacity broadening created by overdense
fibrils could be the main reason for the spectral line broadening observed
frequently in chromospheric fine-scale structures. Spectropolarimetric
inversions of the ViSP data in the Ca II 8542 {\AA} and Fe I 6301/6302 {\AA}
lines are used to construct semiempirical models of the plage atmosphere.
Inversion outputs indicate the existence of dense fibrils in the Ca II 8542
{\AA} line. The analyses of the ViSP data show that the morphological
characteristics, such as orientation, inclination and length of fibrils are
defined by the topology of the magnetic field in the photosphere. Chromospheric
maps reveal a prominent magnetic canopy in the area where fibrils are directed
towards the observer.
