The Rosette Nebula is a well-known H II region shaped by the interaction of gas with the OB stars of the NGC 2244 stellar association. Located within the remnant of a giant molecular cloud, it exhibits a complex structure of ionized gas, molecular material, dust, and embedded clusters. In 2023 October, the region was observed as part of the Sloan Digital Sky Survey V (SDSS-V) local volume mapper (LVM) integral field spectroscopy survey. Covering a radius of $\sim 1^{\circ }$, the data set comprises 33 326 spectra with spatially resolved information spanning 390–980 nm. We present a structural analysis of the ionized, molecular, and dusty components using multiwavelength observations: optical spectroscopy from SDSS-V LVM, $^{12}$CO emission from PMO/MWISP (submillimetre), and dust emission from Wide-field Infrared Survey Explorer ($12 \, \mu \text{m}$) and Herschel (far-infrared). These data sets were complemented with the positions of ionizing stars to study emission structures traced by H $\ALPHA$, H $\BETA$, [O III], [N II], and [S II] as well as the spatial distribution of line ratios (H $\ALPHA$/H $\BETA$, [O III]/H $\BETA$, [N II]/H $\ALPHA$, and [S II]/H $\ALPHA$) relative to the surrounding molecular cloud. Our analysis reveals interaction zones between ionized and neutral gas, including filaments, globules, and dense regions with or without ongoing star formation. Radial and quadrant-based flux profiles further highlight morphological and ionization variations, supporting the scenario in which the Rosette Nebula evolved from a non-homogeneous molecular cloud with a thin, sheet-like structure.